Using the CeSiC material for the WSO-UV spectrographs

Reutlinger, Arnd; Sachkov, Mikhail; Gal, C.; Brandt, C.; Haberler, P.; Zuknik, Karl-Heinz; Sedlmaier, T.; Шустов, Б. М.; Moisheev, A. A.; Kappelmann, N.; Barnstedt, J.; Werner, K.

doi:10.1007/978-94-007-2573-7_44

Cited by 4 publications

(4 citation statements)

References 5 publications

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“…5. The main changes with respect to the previous design (Reutlinger et al 2011) have been: (1) the cross disperser in the UVES spectrograph is now similar to the VUVES spectrograph (based on the cross disperser combined with a UV camera mirror) and (2) segmented toroidal gratings are implemented in the LSS design. CCDs were chosen as detectors for all 3 channels (see Shugarov et al 2014) for more details about the The optical elements of WUVS are being produced by the National Research University of Information Technologies, Mechanics and Optics (ITMO) (see Fig.…”

Section: Wuvs Designmentioning

confidence: 99%

WSO-UV progress and expectations

Шустов

Castro

Sachkov

et al. 2014

Astrophys Space Sci

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Section: Wuvs Designmentioning

confidence: 99%

WSO-UV progress and expectations

Шустов

Castro

Sachkov

et al. 2014

Astrophys Space Sci

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“…2. The main changes with respect to the previous design described above (Reutlinger et al 2011) have been: [1] the cross disperser in the UVES spectrograph is now similar to the VUVES spectrograph (based on the cross disperser combined with a UV camera mirror) and [2] segmented toroidal gratings are implemented in the LSS design. CCDs were chosen as detectors for all 3 channels (see Shugarov et al 2014 for more details about the UV detectors for WUVS).…”

Section: Current Wuvs Designmentioning

confidence: 99%

Optical layouts of the WSO-UV spectrographs

Панчук

Yushkin

Фатхуллин

et al. 2014

Astrophys Space Sci

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World Space Observatory-Ultraviolet project is an international space observatory for spectroscopy and imaging in 115-310 nm spectral range. Significant progress in the CCD development allows to use the back illuminated CCD detectors with anti-reflection coating for observations in this ultraviolet domain instead of MCP detectors. This detector change was one of the main reason for significant correction of layouts of all three WSO-UV spectrographs. In this paper we present the final optical layouts that are now being realized in the WUVS instrument. The using of implemented technological changes in optical layout allows to keep main requirements to WSO-UV spectrographs.

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“…This instrument also used MCP as detector. Cesic material was selected for the spectrograph construction [10].…”

Section: Wuvs: Wso-uv Spectrographsmentioning

confidence: 99%

Instrumentation of the WSO-UV project

2014

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Dedicated to spectroscopic and imaging observations of the ultraviolet sky, the World Space Observatory -Ultraviolet mission is a Russian-Spanish collaboration. The project consists of a 1.7m telescope with instrumentation able to perform: a) high resolution (R ≥50 000) spectroscopy by means of two echellé spectrographs covering the 115-310 nm spectral range; b) long slit (1x75 arcsec) low resolution (R ∼ 1000) spectroscopy with a near-UV channel and a far-UV channel to cover the 115-305 nm spectral range; c) near-UV and a far-UV imaging channels covering the 115-320 nm wavelength range; d) slitless spectroscopy with spectral resolution of about 500 in the full 115-320 nm spectral range.Here we present the WSO-UV focal plane instruments, their status of implementation, and the expected performances.

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Using the CeSiC material for the WSO-UV spectrographs

Cited by 4 publications

References 5 publications

WSO-UV progress and expectations

WSO-UV progress and expectations

Optical layouts of the WSO-UV spectrographs

Instrumentation of the WSO-UV project

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